Zero-metallicity stars I. Evolution at constant mass

By P. Marigo, L. Girardi, C. Chiosi, Peter R. Wood Dip. Astron. Padova, Mssso, Australia. 2001

176 citations recorded by the source corpus.

We present extensive evolutionary models of stars with initial zero-metallicity, covering a large range of initial masses (i.e. 0:7 M M 100 M). Calculations are carried out at constant mass, with updated input physics, and applying an overshooting scheme to convective boundaries. The nuclear network includes all the important reactions of the p-p chain, CNO-cycle and -captures, and is solved by means of a suitable semi-implicit method. The evolution is followed up to the thermally pulsing AGB in the case of low- and intermediate-mass stars, or to the onset of carbon burning in massive stars. The main evolutionary features of these models are discussed, also in comparison with models of non-zero metallicity. Among several interesting aspects, particular attention has been paid to describe: i) the rst synthesis of 12 C inside the stars, that may suddenly trigger the CNO-cycle causing particular evolutionary features; ii) the pollution of the stellar surface by the dredge-up events, that are eective only within particular mass ranges; iii) the mass limits which conventionally dene the classes of low-, intermediate-, and high-mass stars on the basis of common evolutionary properties, including the upper mass limit for the achievement of super-Eddington luminosities before C-ignition in the high-mass regime; and iv) the expected pulsational properties of zero-metallicity stars. All relevant information referring to the evolutionary tracks and isochrones is made available in computer-readable format.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/18cdc9fad97ea93d6050ec90f191b7653758ff2c

Citations in the corpus

• Rates of compact object coalescences (2021, unknown): “Therefore, population III stars may experience reduced radial expansion relative to more metal-rich stars (Marigo et al., 2001) and can avoid mass transfer and many of the complications of the classical isolated binary evolution channel.”
• Possible indirect confirmation of the existence of Pop III massive stars by gravitational wave (2014, unknown): “We find that our fitting formula has an accuracy within 3.5 per cent of the stellar models of Marigo et al. (2001).”
• Theoretical isochrones in several photometric systems. II. The Sloan Digital Sky Survey ugriz system (2004, unknown): “A set for metal-free (Z = 0) stars, from Marigo et al. (2001).”
• On the properties of massive Population III stars and metal-free stellar populations (2001, unknown): “This has also been verified by comparisons of integrated stellar populations adopting alternatively the isochrones provided by Marigo et al. (2001).”
• NUCLEOSYNTHESIS AND EVOLUTION OF MASSIVE METAL-FREE STARS (2008, unknown): “Other recent surveys of zero-metallicity massive stars are Woosley & Weaver (1995), Marigo et al. (2001), Heger & Woosley (2002), Chieffi & Limongi (2004), Umeda & Nomoto (2005), Hirschi et al. (2006), and Tominaga et al. (2007).”
• Evolution and nucleosynthesis of extremely metal-poor and metal-free low- and intermediate-mass stars - I. Stellar yield tables and the CEMPs (2008, unknown): “Cassisi & Castellani 1993; Marigo et al. 2001) and/or have not calculated all of the AGB evolution.”
• GCD+: a new chemodynamical approach to modelling supernovae and chemical enrichment in elliptical galaxies (2002, unknown): “…of the yields for low and zero metallicity stars is important in studies of the chemical composition of extremely metal poor objects observed at both low and high redshifts, although it is not yet wellestablished (e.g. Fujimoto, Ikeda, & Iben 2000; Chieffi, et al. 2001; Marigo et al. 2001).”
• The transition from Population III to normal galaxies: Lyα and He II emission and the ionising properties of high redshift starburst galaxies (2002, unknown): “…we use the following stellar evolution tracks: 1) the Pop III tracks covering masses from 1 to 500 M⊙ with no/negligible mass loss compiled in S02 (Marigo et al. 2001, Feijóo 1999, Desjacques 2000), 2) new main sequence stellar evolution tracks from 1 to 500 M⊙ computed with the Geneva…”
• THE FIRST GALAXIES: CHEMICAL ENRICHMENT, MIXING, AND STAR FORMATION (2010, unknown): “…of this model are that the gas is optically thin to molecule-dissociating radiation, and that the effects of stellar evolution are negligible, which would otherwise lead to a decrease in the number of ionizing photons emitted at the end of the main sequence (Marigo et al. 2001; Schaerer 2002).”
• Stellar evolution with rotation - VIII. Models at Z = 10$^\mathsf{-5}$ and CNO yields for early galactic evolution (2002, unknown): “This feature is also present in zero metallicity stellar models (see e.g. Marigo et al. 2001), but for pop III models, it extends over a broader range of initial masses (from ∼ 10 to ∼ 40 M⊙).”
• CHEMICAL EVOLUTION IN HIERARCHICAL MODELS OF COSMIC STRUCTURE. II. THE FORMATION OF THE MILKY WAY STELLAR HALO AND THE DISTRIBUTION OF THE OLDEST STARS (2009, unknown): “Isochrones with Z = 0 were calculated by Tumlinson et al. (2003) and Marigo et al. (2001); the former did not include ages beyond 108 yr and the latter did not include masses below 0.7 M , so neither provides the complete coverage of age and metallicity that is required by the present models.”
• Evolution of massive Population III stars with rotation and magnetic fields (2012, unknown): “Many authors already addressed these questions using stellar evolution models (Woosley & Weaver 1995; Marigo et al. 2001; Heger & Woosley 2002; Marigo et al. 2003; Chieffi & Limongi 2004; Umeda & Nomoto 2003, 2005; Ekström et al. 2008; Heger & Woosley 2010).”
• Effects of rotation on the evolution of primordial stars (2008, unknown): “Amongst the latest ones, most present the evolution until the AGB phase or central C Article published by EDP Sciences ignition (Chieffi et al. 2001; Marigo et al. 2001, 2003; Siess et al. 2002; Gil-Pons et al. 2007; Lau et al. 2008).”
• Scaled solar tracks and isochrones in a large region of the Z-Y plane I. From the ZAMS to the TP-A (2008, unknown): “…work is basicallythe same as in Bressan et al. (1993), Fagotto et al. (1994a,b) and Girardi et al. (2000), but for updates in the opacities, in the rates of energy loss by plasma neutrinos (see Salasnich et al. 2000), and for the different way the nuclear network is integrated (Marigo et al. 2001).”
• parsec: stellar tracks and isochrones with the PAdova and TRieste Stellar Evolution Code (2012, unknown): “The network of nuclear reactions is solved with a semi-implicit extrapolation scheme (Bader & Deuflhard 1983) that treats all nuclear reactions together and without any assumption on nuclear equilibria (see Marigo et al. 2001).”
• Theoretical isochrones in several photometric systems I. Johnson-Cousins-Glass, HST/WFPC2, HST/NICMOS, Washington, and ESO Imaging Survey filter sets (2002, unknown): “Finally, to this extended set we have included the Marigo et al. (2001) isochrones for zero-metallicity stars.”
• Is HE 0107–5240 A Primordial Star? The Characteristics of Extremely Metal-Poor Carbon-Rich Stars (2004, unknown): “…have been published (Wagner 1974; D’Antona 1982; Guenther & Demarque 1983; Fujimoto et al. 1990, 1995, 2000; Hollowell et al. 1990; Cassisi & Castellani 1993; Cassisi et al. 1996; Weiss et al. 2000; Marigo et al. 2001; Chieffi et al. 2001; Schlattl et al. 2001, 2002; Siess et al. 2002).”
• Scaled solar tracks and isochrones in a large region of the Z-Y plane. II. From 2.5 to 20 solar masses (2009, unknown): “The abundances of the various elements are evaluated with the aid of a semi-implicit extrapolation scheme, as described in Marigo et al. (2001).”